Fig. 3
Eigenfrequencies of precessional modes (solid lines) and their damping (dashed lines) of a compact star with a superfluid component (Sedrakian et al. 1999). The slow mode (upper panel) is normalized to the classical precession frequency ϵΩ, where ϵ is the eccentricity. The fast mode (lower panel) is a fraction of the rotational frequency.
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